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Fig. 10

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Stability regimes in terms of zero-temperature helium white dwarf donor mass versus accretor mass. The upper solid curve is the upper limit for dynamical stability in the presence of an accretion disk that feeds back angular momentum, where almost all transferred matter is lost via isotropic re-emission. The upper dashed curve is the upper stability limit for isotropic re-emission and the lower dashed curve indicates the proposed q = 0.01 lower mass ratio limit for feedback (Sect. 4.1). The lower solid curve encloses the parameter space where systems are dynamically stable in the absence of angular momentum feedback; all matter enters and stays in the disk. The dash-dotted lines indicate when the propeller effect comes into play according to Eq. (31) for several neutron star spin periods and an equatorial magnetic field of 108.5 G. The dotted isochrones indicate the donor masses for system ages (since the onset of mass transfer) of 0.1,1,10   Gyr based on full feedback. The dynamical stability and isotropic re-emission rates are independent of accretor radius and type, hence these curves are continuous. Moreover, the dynamical stability rates are independent of accretor type and therefore also hold for white dwarf accretors.

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